Miao, Jingqi; Sugitani, Koji; White, Glenn J. and Nelson, Richard P.
(2010).
| DOI (Digital Object Identifier) Link: | https://doi.org/10.1088/0004-637X/717/2/658 |
|---|---|
| Google Scholar: | Look up in Google Scholar |
Abstract
We report the results from a smoothed particle hydrodynamics simulation designed to model recent observational data on the nebula and Bright Rim Cloud IC59. We further examine, in the context of radiative-driven implosion (RDI) models, the possible formation mechanisms of the morphological structure of IC59. The results of the simulation reveal the existence of a new, fourth morphological state for Bright Rim Clouds (BRCs)—which we propose to call a TypeMBRC morphology. We discuss the necessary conditions for the appearance of Type MBRCs, based on analytical and numerical simulations. The simulated physical properties from our model are consistent with the available observations of IC59. We further show that the prospect of RDI triggered star formation in all Type M BRCs is not supported by the simulations.
| Item Type: | Article |
|---|---|
| Copyright Holders: | 2010 The American Astronomical Society. |
| ISSN: | 1538-4357 |
| Keywords: | HII regions; kinematics and dynamics; radiative transfer; evolution of stars; star formation |
| Academic Unit/School: | Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences Faculty of Science, Technology, Engineering and Mathematics (STEM) |
| Interdisciplinary Research Centre: | Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR) |
| Item ID: | 24900 |
| Depositing User: | Tracy Bartlett |
| Date Deposited: | 09 Dec 2010 16:43 |
| Last Modified: | 28 Nov 2016 14:46 |
| URI: | http://oro.open.ac.uk/id/eprint/24900 |
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